Manpage of wsrtuvmodel
Section: User Commands (1)
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wsrtuvmodel - Add, subtract, etc, a model from a uv data set.
WSRTUVMODEL is a MIRIAD task which modifies a visibility dataset by a model.
It was derived from the task UVMODEL.
Allowed operations are adding, subtracting, multiplying, dividing and
replacing. The model is specified in the image domain, so that its
Fourier transform is first computed before application to the
visibilities. The model may be either an image (e.g., a CLEAN
component image) or a point source.WSRT
An example is as follows. WSRTUVMODEL could be used to remove CLEAN
components from a visibility data file. The residual data base could
then be examined for anomalous points, which could in turn be clipped.
WSRTUVMODEL could then be reapplied to add the CLEAN components back into
the visibility data base for re-imaging.
Input visibility data file. No default
Input model cube. The default is a point source model.
This will generally be a deconvolved map, formed from the visibility
data being modified. It should be made with ``channel'' linetype.
The model should have units of JY/PIXEL and be weighted by the primary
beam. The task DEMOS can be used to extract primary beam weighted
models from a mosaiced image.
The standard uv selection subcommands. The default is all data.
This gives extra processing options. Several values can be given
(though many values are mutually exclusive), separated by commas.
Option values can be abbreviated to uniqueness.
Possible options are (no default):
add Form: out = vis + model
subtract Form: out = vis - model
multiply Form: out = vis * model
divide Form: out = vis / model
replace Form: out = model
flag Form: out = vis, but flag data where the difference
between vis and model is greater than "sigma" sigmas.
unflag Unflag any flagged data in the output.
mosaic This causes WSRTUVMODEL to select only those visibilities
whose observing center is within plus or minus three
pixels of the model reference pixel. This is needed
if there are multiple pointings or multiple sources in
the input uv file. By default no observing center
selection is performed.
mfs This is used if there is a single plane in the input
model, which is assumed to represen t the data at all
frequencies. This should also be used if the model has
been derived using MFCLEAN.
zero Use the value zero for the model if it cannot be
calculated. This can be used to avoid flagging the
data in the outer parts of the u-v-plane when subtracting
a low resolution model.
The operations add, subtract, multiply, divide, replace and flag are
mutually exclusive. The operations flag and unflag are also mutually
The unflag option should be used with caution. Data in the output
may still be flagged, if it was not possible to calculate the
Clip level. Pixels in the model below this level are set to zero.
The default is not to perform any clipping.
If MODEL is blank, then the flux (Jy) of a point source model should
be specified here. Also used as the default flux in the apriori
option. The default is 1 (assuming the model parameter is not given).
The flux can optionally be followed by i,q,u,v or the other
polarisation mnemonics to indicate the polarisation type.
The RA and DEC offsets (arcseconds) of the point source from the
observing center. A point source to the north and east has positive
offsets. Defaults are zero.
The visibility linetype to use, in the standard form, viz:
Generally if there is an input model, this defaults to the linetype
parameters used to construct the map. For a point source or planet
model, the default is all channels. If you wish to override these
defaults, or if the info is not present in the header, this parameter
can be useful.
For options=flag, WSRTUVMODEL flags those points in the output that
differ by more than "sigma" sigmas. The default is 100.
Output visibility data file name. No default. The output file will
contain only as many channels as there are planes in the model
cube. The various uv variables which describe the windows are
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Time: 18:35:39 GMT, July 05, 2011